In the original formulation of the RS1 model [1]}, [2]}, Randall and Sundrum constructed a consistent solution to the Einstein field equations by choosing a warp factor \(A(\varphi )=k r_c |\varphi |\)  sourced by brane and bulk cosmological constants. Once the Goldberger-Wise mechanism is implemented, such a simple functional form becomes unavailable: the background geometry is augmented, the Einstein field equations are changed, and the warp factor \(A(\varphi )\)  is made more complicated. The background Einstein field equations of the stabilized model (Eqs. (REF ), (REF ), (REF ), and (REF )) are coupled non-linear equations with respect to \(A(\varphi )\)  that depend on the derivative of the scalar background \(\phi _{0}^{\prime }(\varphi )\)  and are generally difficult to solve.
DeWolfe, Freedman, Gubser, and Karch have constructed a specific class of exactly solvable potentials (the DFGK model) [3]} which make calculations in the stabilized RS1 model feasible.
